adsabs/AstroCLIMB huggingface dataset:
Paper: Locating Hidden Exoplanets in ALMA Data Using Machine Learning
Authors: J. P. Terry, C. Hall, S. Abreau, S. Gleyzer
Figure caption: Example raw (top row) and convolved, noisy (bottom row) channel maps in a disk with a planet present. The planet (circled in white) is visible as a kink in the right column. The opposite velocity channel is shown in the left column, and the systemic channel is shown in the middle column. The beam size is indicated in the bottom middle image (solid white circle). This disk is one of the smallest and farthest simulated and is observed with some of the worst spatial resolutions, which is why the beam is so large.
Paper: Locating Hidden Exoplanets in ALMA Data Using Machine Learning
Authors: J. P. Terry, C. Hall, S. Abreau, S. Gleyzer
Figure caption: Example raw (top row) and convolved, noisy (bottom row) channel maps in a disk without a planet present. The beam size is indicated in the bottom middle image.
Paper: An Elusive Population of Massive Disk Galaxies Hosting Double-lobed Radio-loud Active Galactic Nuclei
Authors: Zihao Wu, Luis C. Ho, Ming-Yang Zhuang
Figure caption: Radio luminosity–BH mass relation showing the FR I–FR II dichotomy. The top x-axis gives the total stellar mass. The right y-axis converts radio luminosity to jet power following Equation (10). The solid line is the BH mass version of the Owen–Ledlow relation, where we converted the R-band absolute magnitude to BH mass as described in Section 5.2. The dashed lines show constant critical ratios of jet power over Eddington luminosity, α ≡ P jet/L Edd = 1, 0.1, and 0.005. Large filled circles are objects from our sample, stars are objects from the literature (Table 5), and small open circles are elliptical galaxies from Owen & Ledlow (1994).
Paper: An Elusive Population of Massive Disk Galaxies Hosting Double-lobed Radio-loud Active Galactic Nuclei
Authors: Zihao Wu, Luis C. Ho, Ming-Yang Zhuang
Figure caption: Distribution of (a) concentration parameter C, (b) bulge-to-total light ratio B/T, (c) global Sérsic index n global, and (d) bulge Sérsic index n bulge for our sample of disk radio galaxies, in comparison with the control sample of normal galaxies from CGS (blue symbols, spirals; red symbols, ellipticals; Li et al. 2011; Gao et al. 2019). The irregular galaxy J0802+115 and the dwarf Magellanic spiral galaxy J1328+571, which do not have a bulge, are not shown in panels (b) and (d). All quantities pertain to the R band.
Paper: An Elusive Population of Massive Disk Galaxies Hosting Double-lobed Radio-loud Active Galactic Nuclei
Authors: Zihao Wu, Luis C. Ho, Ming-Yang Zhuang
Figure caption: (a) Probability density as a function of the g-band absolute magnitude for red galaxies from Loveday et al. (2012). (b) Predicted probability density as a function of the redshift for galaxies with radio lobes and S tot = 50 mJy. (c) Cumulative probability distribution of a potential elliptical host of radio lobes as a function of the g-band apparent magnitude. Histograms denote objects with detected radio lobes and S tot = 30–70 mJy (Sadler et al. 2002).
Paper: An Elusive Population of Massive Disk Galaxies Hosting Double-lobed Radio-loud Active Galactic Nuclei
Authors: Zihao Wu, Luis C. Ho, Ming-Yang Zhuang
Figure caption: Examples of two-dimensional bulge–disk decomposition using GALFIT. The left column shows the surface brightness profile of the data (open circles with error bars), Sérsic bulge component (red), exponential disk component (blue), and total (bulge + disk) model (purple). The ﹩{\chi }_{\nu }^{2}﹩ from GALFIT is shown in the lower-left corner. The lower panel gives the residuals between the data and the model. The right three columns show the original data, best-fit total model, and residuals, respectively. All images are displayed on a log stretch.
Paper: An Elusive Population of Massive Disk Galaxies Hosting Double-lobed Radio-loud Active Galactic Nuclei
Authors: Zihao Wu, Luis C. Ho, Ming-Yang Zhuang
Figure caption: Radio–optical luminosity relation showing the FR I–FR II dichotomy. The solid line is the Owen–Ledlow relation that divides FR I (red) and FR II (blue) sources. Large filled circles are objects from our sample, stars are objects from the literature (Table 5), and small open circles are elliptical galaxies from Owen & Ledlow (1994).
Paper: An Elusive Population of Massive Disk Galaxies Hosting Double-lobed Radio-loud Active Galactic Nuclei
Authors: Zihao Wu, Luis C. Ho, Ming-Yang Zhuang
Figure caption: Distribution of bulges of host galaxies in the Kormendy relation. The black solid line shows the Kormendy relation measured in the R band from Gao et al. (2020), with the shaded region showing the 3σ range. Classical bulges and ellipticals follow the Kormendy relation, while pseudobulges are low-surface brightness outliers below the relation. The HST F475W magnitudes have been K-corrected to the R band.
Paper: An Elusive Population of Massive Disk Galaxies Hosting Double-lobed Radio-loud Active Galactic Nuclei
Authors: Zihao Wu, Luis C. Ho, Ming-Yang Zhuang
Figure caption: Effective radius (r  e ) vs. stellar mass (M *) for the host galaxies of the double-lobed radio sources in our sample, with colors indicating their bulge-to-total light ratios (B/T). The blue and red solid lines represent the mass–size relations of star-forming and quiescent galaxies at z ≈ 0.2−0.4 (Kawinwanichakij et al. 2021), with shaded areas indicating the 1σ intrinsic scatter of ﹩\mathrm{log}{r}_{e}﹩.
Paper: An Elusive Population of Massive Disk Galaxies Hosting Double-lobed Radio-loud Active Galactic Nuclei
Authors: Zihao Wu, Luis C. Ho, Ming-Yang Zhuang
Figure caption: [O III]/Hβ vs. (a) [N II]/Hα and (b) [S II]/Hα diagnostic diagrams for objects with signal-to-noise ratios larger than 2 in their optical emission-line fluxes. The extreme starburst boundary (red solid line; Kewley et al. 2001), the pure star formation line (blue dashed line in panel a; Kauffmann et al. 2003), and the separation between Seyferts and LINERs (green dotted line in panel b; Kewley et al. 2006) are used to classify galaxies into star-forming (H II) galaxies, Seyferts, LINERs, and composite (star-forming and AGN) systems.
Paper: A Stochastic Theory of the Hierarchical Clustering. III. The Nonuniversality and Nonstationarity of the Halo Mass Function
Authors: Andrea Lapi, Tommaso Ronconi, Luigi Danese
Figure caption: Fits to the halo multiplicity function by Shirasaki et al. (2021) at z ≈ 0 (circles) with the stationary solution of the Fokker–Planck equation (see Equation (14); blue solid line), and with the excursion set approach (see Equation (16); red line). The Press & Schechter (1974) multiplicity function is also reported for reference (green lines). The nonuniversal behavior in the simulations is highlighted by the different shapes of the multiplicity function by Shirasaki et al. (2021) at z ≈ 3 (squares). The inset shows the deviation of the noise strength (for the stochastic theory) or of the collapse threshold (excursion set) from the constant case yielding the Press & Schechter (1974) shape.
Paper: A Stochastic Theory of the Hierarchical Clustering. III. The Nonuniversality and Nonstationarity of the Halo Mass Function
Authors: Andrea Lapi, Tommaso Ronconi, Luigi Danese
Figure caption: MCMC posterior distributions for the parameters triple (q, β, γ) ruling the mass/redshift dependence in Equation (8), obtained by fitting the halo multiplicity function at z ≈ 0 by Shirasaki et al. (2021) via the stationary solutions of the Fokker–Planck equation (blue contours/lines; see Equation (14)), and via the excursion set approach (red contours/lines; see Equation (16)). Contours show 68% and 95% confidence intervals, and the marginalized distributions are in arbitrary units (normalized to 1 at their maximum value).
Paper: A Stochastic Theory of the Hierarchical Clustering. III. The Nonuniversality and Nonstationarity of the Halo Mass Function
Authors: Andrea Lapi, Tommaso Ronconi, Luigi Danese
Figure caption: MCMC posterior distributions for the parameters triple (q, β, γ) ruling the mass/redshift dependence in Equation (8) and the initial condition ν in set at z in ≈ 100, obtained by fitting the halo multiplicity function by Shirasaki et al. (2021) in the redshift range z ≈ 0–3 via the time-dependent solutions of the Fokker–Planck equation (green contours/lines; see Equation (13)). For comparison, the posterior distributions on (q, β, γ) for the fit via the stationary solution of the Fokker–Planck equation are reported in Figure 1 (blue contours/lines). Contours show 68% and 95% confidence intervals, and the marginalized distributions are in arbitrary units (normalized to 1 at their maximum value).
Paper: A Stochastic Theory of the Hierarchical Clustering. III. The Nonuniversality and Nonstationarity of the Halo Mass Function
Authors: Andrea Lapi, Tommaso Ronconi, Luigi Danese
Figure caption: The overall evolution of the time-dependent solutions of the Fokker–Planck equation; fitting parameters (q, β, γ, ν in) have been set at the mean posterior values from the previous Figure (see also Table 1). Colored lines are for different redshifts from z in ≈ 100 down to z ≈ 0 as illustrated by the color bar. The magenta line shows the corresponding stationary state.
Paper: A Molecular Gas Ring Hidden in the Sombrero Galaxy
Authors: Jessica Sutter, Dario Fadda
Figure caption: The [C II]/FIR ratio plotted as a function of far-IR surface brightness (ΣFIR). The regions within M 104 are color-coded based on their position in the BPT diagram as in previous figures. The comparison data from NGC 7331 (Sutter & Fadda 2022), KINGFISH (star-forming regions in local galaxies from Sutter et al. (2019)), z ∼ 0.02–0.2 galaxies from Ibar et al. (2015), and local U/LIRGS (Díaz-Santos et al. 2017) are shown in gray, light gray, brown, and light brown, respectively. We also include global measurements from local early-type galaxies (ETGs) in magenta, and the global measurement of M104 as a magenta star.
Paper: A Molecular Gas Ring Hidden in the Sombrero Galaxy
Authors: Jessica Sutter, Dario Fadda
Figure caption: Two examples of the spectral energy distribution fits produced by CIGALE: the nucleus (top) and the S1 region on the ring (bottom). Data are marked by blue points, and the total model flux is plotted in gray. Magenta and cyan lines show the unattenuated light from the old and young stellar populations, respectively. The dust component is displayed in red, while the AGN emission in plotted in orange. In the nucleus, the young stellar population is negligible and the AGN produces a large percentage of the near- to mid-infrared flux. On the other hand, in the ring there is a substantial population of young stars and the IR emission is well-fit without any AGN component.
Paper: A Molecular Gas Ring Hidden in the Sombrero Galaxy
Authors: Jessica Sutter, Dario Fadda
Figure caption: Line-of-sight velocity along the ring for the optical, [C II], and CO emissions as a function of the projected distance from the galaxy center. The error bars correspond to 3σ errors. The different measurement sets have been spaced for clarity by 100 km s−1 intervals. In the legend, XC and EM stand for cross-correlation and emission lines, the two methods used to estimate redshifts from the optical spectra. The inset displays the ellipses of confidence for the four linear fits at the 1σ, 2σ, and 3σ levels (the 39%, 86%, and 99% levels of confidence for two variables; see, e.g., Wang et al. 2015).
Paper: A Molecular Gas Ring Hidden in the Sombrero Galaxy
Authors: Jessica Sutter, Dario Fadda
Figure caption: Surface brightness of the [C II] line plotted as a function of the attenuated UV light from the CIGALE SED fits. M104 data are color-coded based on the BPT diagram diagnostic, with orange being star-forming, and green being dominated by LIERs. The LIERs are further divided into regions interior to the ring (dark green) and along the ring (light green). Comparison data from the nearby galaxy NGC 7331, our ETG sample, and M 31 are shown as gray, magenta, and purple symbols, respectively. The global M104 measurement is shown as a magenta star. Median error bars, scaled to be the correct size on this plot at the locus of the data from M 104, are shown in the right bottom corner.
Paper: A Molecular Gas Ring Hidden in the Sombrero Galaxy
Authors: Jessica Sutter, Dario Fadda
Figure caption: A Kennicutt–Schmidt plot with star formation rate surface density plotted against the molecular gas surface density. The relationship for sub-Kpc regions in star-forming galaxies from Bigiel et al. (2008) is shown as a blue line, with blue shading representing the 3σ error on the slope. Data for NGC 7331 (Sutter & Fadda 2022) are marked with gray dots. Median error bars for the data from M104 (orange and green diamonds) are shown as a black cross in the lower part of the plot.
Paper: A Molecular Gas Ring Hidden in the Sombrero Galaxy
Authors: Jessica Sutter, Dario Fadda
Figure caption: Emission line diagnostic diagrams used to identify LIER and star-forming regions. The regions are labeled as Seyfert (Sy), H II, Composite (Comp), and LIER. Median error bars are shown in the right bottom corner.
Paper: A Molecular Gas Ring Hidden in the Sombrero Galaxy
Authors: Jessica Sutter, Dario Fadda
Figure caption: The [C II]/PAH values, now plotted against the ratio of the 7.7  μm and 11.3 μm PAH features, an indicator of PAH charge. Same color scheme as previous plot. Histograms above and to the right show the distribution of the different types of regions in M 104 with respect to the star-forming galaxy sample. Median error bars for the data from M104 are shown in the lower-right corner.
Paper: A Molecular Gas Ring Hidden in the Sombrero Galaxy
Authors: Jessica Sutter, Dario Fadda
Figure caption: The [C II]/PAH values plotted as a function of ﹩{(\nu {F}_{\nu })}_{70\mu {\rm{m}}}/{(\nu {F}_{\nu })}_{100\mu {\rm{m}}}﹩. The points from M 104 follow the color scheme of previous plots. Resolved measurements from three nearby star-forming galaxies, NGC 7331, NGC 4559, and NGC 1097 (Croxall et al. 2012; Sutter & Fadda 2022), are shown as gray points. Median error bars for M104 are shown on the left.
Paper: A Molecular Gas Ring Hidden in the Sombrero Galaxy
Authors: Jessica Sutter, Dario Fadda
Figure caption: CO luminosities plotted against the [C II] luminosities, both normalized by the FIR luminosity. Median error bars for the data from M104 are shown in the lower left corner.
Paper: Exploring Realistic Nanohertz Gravitational-wave Backgrounds
Authors: Bence Bécsy, Neil J. Cornish, Luke Zoltan Kelley
Figure caption: Location of the loudest sources on the h  c –f obs plane over 500 realizations of the binary population with 100 random extrinsic parameters each (50,000 in total). The color of each circle indicates the S/N of the loudest source in the particular realization. Note that the color scale was capped at S/N = 5 for better visibility. We also show the GWB spectra for each realization in blue. Sources can have significant S/Ns even if they are below the characteristic strain spectrum for the GWB if they have favorable extrinsic parameters (e.g., sky locations and inclinations).
Paper: Exploring Realistic Nanohertz Gravitational-wave Backgrounds
Authors: Bence Bécsy, Neil J. Cornish, Luke Zoltan Kelley
Figure caption: Distribution of S/Ns for a particular source. The top panel shows the overall distribution (gray), along with histograms restricted to the half of the sky centered on the most sensitive sky location (red) and the antipodal point (blue). The bottom panel shows how S/N correlates with the orbital inclination (ι). The coloring indicates each source’s angular distance from the most sensitive sky location (see black cross in Figure 11).
Paper: Numerical Simulations of Oscillations in Solar Corona Excited by Vortex Shedding
Authors: Petr Jelínek, Sofya Belov, Marian Karlický
Figure caption: The sketch of the numerical box. The box size is (−2.5, 2.5) × (−2.5, 2.5) Mm in a horizontal direction and (0, 20) Mm in a vertical direction. The blue cylinder represents the obstacle with internal magnetic field B i; external magnetic field is B e. The initial flow is denoted as v  z0.
Paper: Exploring Realistic Nanohertz Gravitational-wave Backgrounds
Authors: Bence Bécsy, Neil J. Cornish, Luke Zoltan Kelley
Figure caption: Distribution of the detector-frame GW frequency and chirp mass, luminosity distance, inclination angle, and S/N of the loudest source over 500 binary population realizations with 100 realizations each (50,000 in total). Dashed lines and quoted values correspond to the 5th/50th/95th percentiles. Gray histograms show all realizations, while red histograms show only those where the S/N is larger than 5 (∼8% of all realizations).
Paper: Numerical Simulations of Oscillations in Solar Corona Excited by Vortex Shedding
Authors: Petr Jelínek, Sofya Belov, Marian Karlický
Figure caption: The set of figures showing the y-component of vorticity ω, in arbitrary units, for initial flow speed v  z0 = 89 km s−1, at time t  =  1120 s for different values of the magnetic field. The strength of magnetic field is from 1 to 5 G (left to the right), respectively.
Paper: Exploring Realistic Nanohertz Gravitational-wave Backgrounds
Authors: Bence Bécsy, Neil J. Cornish, Luke Zoltan Kelley
Figure caption: Variance of HD correlations from a CW simulation without pulsar terms and a simulated PTA with isotropically distributed pulsars. We also show the theoretical variance with two different averaging procedures described in Section A.1.
Paper: Exploring Realistic Nanohertz Gravitational-wave Backgrounds
Authors: Bence Bécsy, Neil J. Cornish, Luke Zoltan Kelley
Figure caption: Variance of HD correlations from a CW simulation with pulsar terms and a simulated PTA with isotropically distributed pulsars. We also show the theoretical variance with two different averaging procedures described in Section A.2.
Paper: Numerical Simulations of Oscillations in Solar Corona Excited by Vortex Shedding
Authors: Petr Jelínek, Sofya Belov, Marian Karlický
Figure caption: The dependence of vortex period (a) and Strouhal number (b) on the value of magnetic field.
Paper: A Very Large Array Study of Newly Discovered Southern Latitude Nonthermal Filaments in the Galactic Center: Radio Continuum Total-intensity and Spectral Index Properties
Authors: Dylan M. Paré, Cornelia C. Lang, Mark R. Morris
Figure caption: 6 GHz total-intensity distribution of SNTF1 (G0.30-0.26). This image has a beam size of 4.″1 × 2.″1 and an rms noise level of ∼100 μJy beam−1. The yellow rectangle indicates the intersection of SNTF1 with the oblique filament as discussed in the text. Key features are labeled in the image.
Paper: A Very Large Array Study of Newly Discovered Southern Latitude Nonthermal Filaments in the Galactic Center: Radio Continuum Total-intensity and Spectral Index Properties
Authors: Dylan M. Paré, Cornelia C. Lang, Mark R. Morris
Figure caption: 1 GHz MeerKAT image of the GC (Heywood et al. 2022; Yusef-Zadeh et al. 2022) with the VLA fields of view for our NTFB observations overlayed as circles. The X-band fields of view are in blue and the C-band fields of view are in green. The black rectangle indicates the field of view of our previous Radio Arc observations (Paré et al. 2019, 2021).
Paper: Unusual Abundances from Planetary System Material Polluting the White Dwarf G238-44
Authors: Ted M Johnson, Beth L. Klein, D. Koester, Carl Melis, B. Zuckerman, M. Jura
Figure caption: Elemental abundance ratios by number for the material polluting G238-44 compared to other WDs, solar system bodies, and the two-body model we propose in Section 4.2. Abundances from: Bulk Earth—Allègre et al. (2001), Mercury—Brugger et al. (2018); Nittler et al. (2018), Comet Halley dust—Jessberger et al. (1988), 67P/ChuryumovGerasimenko—Bardyn et al. (2017), Solar & CI Chondrite—Lodders (2021), G200-39—Xu et al. (2017), GD 378—Klein et al. (2021). O is an incredibly versatile element when it comes to planet formation. It is a significant component of any solar system object. However, C, N, and Fe are much more specialized. Fe abundance is high in objects that formed close to their parent star. In contrast, N can only form in significant amounts past the ice line. We do not expect objects that are high in Fe to also be high in N. G238-44 breaks this trend and has both high Fe/O and N/O. The proposed two-body model is capable of reproducing this unusual characteristic.
Paper: Unusual Abundances from Planetary System Material Polluting the White Dwarf G238-44
Authors: Ted M Johnson, Beth L. Klein, D. Koester, Carl Melis, B. Zuckerman, M. Jura
Figure caption: Reduced χ 2 fits exploring two-body models; note that the y-axis is log10. Only atomic abundance information is incorporated into these model tests; i.e., the presence of metallic and icy material is not assessed by the χ 2 fit. We find that a mix of metal-dominated Mercury-like material and icy Kuiper Belt object-like material (G200-39; see text) in a ratio of 1.7:1 provides the best fit to the data.
Paper: Unusual Abundances from Planetary System Material Polluting the White Dwarf G238-44
Authors: Ted M Johnson, Beth L. Klein, D. Koester, Carl Melis, B. Zuckerman, M. Jura
Figure caption: Residuals for elemental abundances (expressed as a percentage of the total parent body mass) when comparing G238-44 and various parent body models. The two-body model, informed from the best fit in Figure 7 and discussed in Section 4.2, fits within the errors both for Fe and ices (C, N, and O). Single-body models are not reasonable matches to the data.
Paper: Unusual Abundances from Planetary System Material Polluting the White Dwarf G238-44
Authors: Ted M Johnson, Beth L. Klein, D. Koester, Carl Melis, B. Zuckerman, M. Jura
Figure caption: Carbon lines found in FUSE spectra. See Section 3.4.1.
Paper: Unusual Abundances from Planetary System Material Polluting the White Dwarf G238-44
Authors: Ted M Johnson, Beth L. Klein, D. Koester, Carl Melis, B. Zuckerman, M. Jura
Figure caption: HIRES spectra showing all detected lines (except Ca II λ3968 which lies within the Hϵ Balmer transition). The model with the best-fit abundances is overplotted in red.
Paper: The Astrometric Animation of Water Masers toward the Mira Variable BX Cam
Authors: Shuangjing Xu, Hiroshi Imai, Youngjoo Yun, Bo Zhang, María J. Rioja, Richard Dodson, Se-Hyung Cho, Jaeheon Kim, Lang Cui, Andrey M. Sobolev, James O. Chibueze, Dong-Jin Kim, Kei Amada, Jun-ichi Nakashima, Gabor Orosz, Miyako Oyadomari, Sejin Oh, Yoshinori Yonekura, Yan Sun, Xiaofeng Mai, Jingdong Zhang, Shiming Wen, Taehyun Jung
Figure caption:                         The morphology of individual maser features. The color and size of maser spots are the same as in Figure 14.
Paper: The Astrometric Animation of Water Masers toward the Mira Variable BX Cam
Authors: Shuangjing Xu, Hiroshi Imai, Youngjoo Yun, Bo Zhang, María J. Rioja, Richard Dodson, Se-Hyung Cho, Jaeheon Kim, Lang Cui, Andrey M. Sobolev, James O. Chibueze, Dong-Jin Kim, Kei Amada, Jun-ichi Nakashima, Gabor Orosz, Miyako Oyadomari, Sejin Oh, Yoshinori Yonekura, Yan Sun, Xiaofeng Mai, Jingdong Zhang, Shiming Wen, Taehyun Jung
Figure caption:                         Temporal variation of maser features in different regions. The locations of the different regions are shown in Figure 4, while Region 1 includes MF[1,2,3,17], Region 2 includes MF[4,13,14,15], Region 3 includes MF[5,6], and Region 4 includes MF[7,8,9,10,11,12]. The velocity gradient is classified by color, and the size of the maser spots represents the flux density. The color and size of maser spots are the same as in Figure 14. The optical light curve is plotted using the AAVSO photometric data (blue stars).
Paper: Herschel Optimized Tau and Temperature (HOTT) Maps: Uncertainty Analysis and Robust Parameter Extraction
Authors: Ayushi Singh, Peter G. Martin
Figure caption: Top: HSA 70 μm map of Perseus E, convolved to 500 μm resolution and with an approximate zero-level correction. Bottom: extrapolated 70 μm map from the HOTT thermal dust model.